The fact that the universe is in a state of accelerated expansion today is supported by the observational evidence from various cosmological tools such as the Cosmic Microwave Background (CMB), Type 1a Supernovae (SN1a), and Baryon Acoustic Oscillations (BAO)[1]}. The increasing rate of expansion is attributed to an unknown cosmological component called Dark Energy, which constitutes around 70% of the total energy density of the current universe. Current data shows Dark Energy began to affect the dynamics of the universe around a redshift of z \(\sim \)  2 (10.5 Gyr ago), and became the dominant component of the energy density at around a redshift of z \(\sim \)  0.5 (5.2 Gyr ago). Constraining the properties of Dark Energy, and the evolution of the universe over cosmic timescales, is an important goal of modern cosmology.
